Linear Mode Decomposition in Magnetohydrodynamics Revisited
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F23%3A10475999" target="_blank" >RIV/00216208:11320/23:10475999 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=JowiUmc6m8" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=JowiUmc6m8</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/1538-4365/acdf5d" target="_blank" >10.3847/1538-4365/acdf5d</a>
Alternative languages
Result language
angličtina
Original language name
Linear Mode Decomposition in Magnetohydrodynamics Revisited
Original language description
Small-amplitude fluctuations in the magnetized solar wind are measured typically by a single spacecraft. In the magnetohydrodynamics (MHD) description, fluctuations are typically expressed in terms of the fundamental modes admitted by the system. An important question is how to resolve an observed set of fluctuations, typically plasma moments such as the density, velocity, pressure, and magnetic field fluctuations, into their constituent fundamental MHD modal components. Despite its importance in understanding the basic elements of waves and turbulence in the solar wind, this problem has not yet been fully resolved. Here, we introduce a new method that identifies between wave modes and advected structures such as magnetic islands or entropy modes and computes the phase information associated with the eligible MHD modes. The mode-decomposition method developed here identifies the admissible modes in an MHD plasma from a set of plasma and magnetic field fluctuations measured by a single spacecraft at a specific frequency and an inferred wavenumber k(m). We present data from three typical intervals measured by the Wind and Solar Orbiter spacecraft at similar to 1 au and show how the new method identifies both propagating (wave) and nonpropagating (structures) modes, including entropy and magnetic island modes. This allows us to identify and characterize the separate MHD modes in an observed plasma parcel and to derive wavenumber spectra of entropic density, fast and slow magnetosonic, Alfvenic, and magnetic island fluctuations for the first time. These results help identify the fundamental building blocks of turbulence in the magnetized solar wind.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10305 - Fluids and plasma physics (including surface physics)
Result continuities
Project
<a href="/en/project/GA23-06401S" target="_blank" >GA23-06401S: Where and how the solar wind is accelerated and heated and how these processes affect its evolution?</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2023
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal, Supplement Series
ISSN
0067-0049
e-ISSN
1538-4365
Volume of the periodical
268
Issue of the periodical within the volume
1
Country of publishing house
US - UNITED STATES
Number of pages
38
Pages from-to
18
UT code for WoS article
001056792900001
EID of the result in the Scopus database
2-s2.0-85170074780